Welcome to PACMAN
PACMAN is a pipeline to reduce and analyze Hubble/Wide Field Camera 3 (WFC3) observations of transiting exoplanets. The pipeline runs end-to-end, beginning with a time series of 2D images and ending with a spectrum for the planet. PACMAN can easily fit multiple observations simultaneously.
The main steps in the pipeline are:
- optimally extract spectra from the 'ima' data products provided by STScI
- bin the spectra into user-specified wavelength bins and output the light curve(s)
- fit the light curves with a variety of astrophysical models (transit, eclipse, phase curve) and instrument systematic models (visit-long quadratic trends, orbit-long exponential trends)
- estimate uncertainties on the planet parameters with least-squares, MCMC, or nested sampling
Check out the docs for the latest instructions for how to install and use PACMAN.
If you are encountering issues with the code, please take a look at the issues page to see if anyone else has encountered similar problems (make sure you check both open and closed GitHub Issues!).
If not, raise an issue and we will do our best to address it!
When submitting an issues, please provide information like the current PACMAN version and the error message you are receiving in your terminal.
Also, have a look at our FAQ page where we collect frequently asked questions.
If you are thinking about contributing to PACMAN, please also create an issue, so that we can make sure nobody else is already working on the same feature.